ESSnuSB / ESSnuSB+

Funded by the European Union

$fractal-1120768_1920-compressor optimised$
ESSνSB proton accelerator Power (5MW):

Image by Pete Linforth on Pixabay

5.5 times the power of the most powerful road-going car Bugatti Veyron Super.
It will take the ESSνSB Super Beam proton pulse 1.8 ms=0.0018 seconds to reach the far detector if located at 540 km distance from ESS (Garpenberg mine) or 1.2ms=0.0012 seconds if located at 360km (Zinkgruvan mine).

Image by Pete Linforth on Pixabay
ESSνSB Far Detector will be built 1km underground which is at a depth of about 3 times the height of the Eiffel Tower.

Picture by Gerd Altmann on Pixabay
$fractal-1746832_1920-compressor optimised$
The ESS Linear Accelerator (Linac) is 490m long which represents around 4.7 times the length of a soccer field.

Picture by Garik Barseghyan on Pixabay
ESSνSB Far Detector will contain 1 000 000 000 litres of water which represents a volume equal to that of a cube 100 m high and with a 100 m x 100 m bottom surface and is twice the volume that can be carried by the world largest super-tanker (TI Europe)

Picture by Kai Kalhh on Pixabay
ESSνSB is the world's most intense neutrino beam project.

Picture by Media Design and Media Publishing on Pixabay
What are neutrinos?

Picture by Gerd Altmann on Pixabay

The lightest fundamental particle.
Neutrinos are elusive and difficult to detect.

Picture by Gerd Altmann on Pixabay
Neutrinos are plentiful: they come from everywhere, from the sun, from the earth, from supernovae and from the Big Bang.

Image by Barbara A. Lane on Pixabay
Neutrinos travel as fast as light (almost!)

Picture by Public Domain Pictures on Pixabay
Neutrinos have three different flavours: Electron, Muon, Tau.

Picture by Gerd Altmann on Pixabay
Without the asymmetry between Matter and Antimatter we would not exist. How this symmetry was broken is an outstanding question?

Picture by Gerd Altmann of Pixabay

ESSνSB will study this question.
The years of major neutrino discoveries and years when those discoveries were awarded the Nobel Prizes:

Picture by Gerd Altmann on Pixabay

Pauli 1930/1945 : Prediction of neutrino

Cowan & Reines 1956/1995: Discovery of neutrino.

Davis & Koshiba 1987/2002: Solar & cosmic neutrinos.

Kajita & McDonald 1998/2001/2015: Neutrino oscillations.
ESSνSB Timeline and funding obtained (till 2017) or required (as of 2022):

Picture by Gerd Altmann on Pixabay

2015: Concept (2M€)

2019: Initial Design (5M€)

2022: Final Design (10M€)

2025: Construction of Detector (550M€)

2028: Construction of Neutrino Source (650M€)

2035-2085: Operational phase

2012: First ideas
There were equal quantities of Matter and Antimatter created in the Big Bang.

Image by Douglas James on Pixabay

But there is no antimatter in the Universe now. Why?
$fractal-1280081_1920-slider optimised$
Advantages of ESSνSB Project:

Image by Douglas James on Pixabay

- Hightest production intensity (5MW proton driver);

- Largest detector (1 million tonnes of water);

- Greatest sensitivity (measures at the 2nd neutrino oscillation maximum).
Picture by Wikilmages on Pixabay

In ESSνSB project, a single beam pulse has the same energy as a 7.2kg bullet traveling at 1100 km/hour or, differently expressed, has the same kinetic energy as a 1000 kg car traveling at nearly 100 km/hour or the same heat energy it takes to melt 1000 kg of ice.
Picture by Wikilmages on Pixabay

In the ESSνSB project, the duration of a super beam pulse will be 3 ms which means that there will be a distance of 900km (distance between Roma in Italy and Geneva in Switzerland) between the first and the last proton of the beam pulse.